The effects of near ultraviolet (UV) radiation on water solutions of tyrosine and glycine-tyrosine are investigated using a broadband xenon lamp in the region 200–800 nm. These experiments form a contribution in the laboratory simulation of the solar irradiation on the building blocks of life with regard to the origin of life. Results are presented showing the photodecomposition of tyrosine and glycine-tyrosine, at different concentrations, against UV doses. The analysis of the irradiated solutions is carried out by spectroscopic and analytical techniques. The findings of our laboratory simulations are used to constrain the early stages of the life emerging process.

All known life requires phosphorus (P) in the form of inorganic phosphate (PO43− or Pi) and phosphate-containing organic molecules. Pi serves as the backbone of the nucleic acids that constitute genetic material and as the major repository of chemical energy for metabolism in polyphosphate bonds. Arsenic (As) lies directly below P on the periodic table and so the two elements share many chemical properties, although their chemistries are sufficiently dissimilar that As cannot directly replace P in modern biochemistry. Arsenic is toxic because As and P are similar enough that organisms attempt this substitution. We hypothesize that ancient biochemical systems, analogous to but distinct from those known today, could have utilized arsenate in the equivalent biological role as phosphate. Organisms utilizing such ‘weird life’ biochemical pathways may have supported a ‘shadow biosphere’ at the time of the origin and early evolution of life on Earth or on other planets. Such organisms may even persist on Earth today, undetected, in unusual niches.

It has long been assumed that the planet Jupiter acts as a giant shield, significantly lowering the impact rate of minor bodies upon the Earth, and thus enabling the development and evolution of life in a collisional environment which is not overly hostile. In other words, it is thought that, thanks to Jupiter, mass extinctions have been sufficiently infrequent that the biosphere has been able to diversify and prosper. However, in the past, little work has been carried out to examine the validity of this idea. In the second of a series of papers, we examine the degree to which the impact risk resulting from objects on Centaur-like orbits is affected by the presence of a giant planet, in an attempt to fully understand the impact regime under which life on Earth has developed. The Centaurs are a population of ice-rich bodies which move on dynamically unstable orbits in the outer Solar system. The largest Centaurs known are several hundred kilometres in diameter, and it is certain that a great number of kilometre or sub-kilometre sized Centaurs still await discovery. These objects move on orbits which bring them closer to the Sun than Neptune, although they remain beyond the orbit of Jupiter at all times, and have their origins in the vast reservoir of debris known as the Edgeworth–Kuiper belt that extends beyond Neptune. Over time, the giant planets perturb the Centaurs, sending a significant fraction into the inner Solar System where they become visible as short-period comets. In this work, we obtain results which show that the presence of a giant planet can act to significantly change the impact rate of short-period comets on the Earth, and that such planets often actually increase the impact flux greatly over that which would be expected were a giant planet not present.

The so-called vegetation red-edge (VRE), a sharp increase in the reflectance around 700 nm, is a characteristic of vegetation spectra, and can therefore be used as a biomarker if it can be detected in an unresolved extrasolar Earth-like planet integrated reflectance spectrum. Here, we investigate the potential for the detection of vegetation spectra during the last Quaternary climatic extrema, the Last Glacial Maximum (LGM) and the Holocene optimum, for which past climatic simulations have been made. By testing the VRE detectability during these extrema, when Earth's climate and biomes maps were different from today, we are able to test the vegetation detectability on a terrestrial planet different from our modern Earth. Data from the Biome3.5 model have been associated to visible Global Ozone Monitoring Experiment (GOME) spectra for each biome and cloud cover to derive Earth's integrated spectra for given Earth phases and observer positions. The VRE is then measured. Results show that the vegetation remains detectable during the last climatic extrema. Compared to the current Earth, the Holocene optimum, with a greener Sahara, slightly increases the mean VRE on one hand, while on the other hand, the large ice cap over the northern hemisphere during the LGM decreases vegetation detectability. We finally discuss the detectability of the VRE in the context of recently proposed space missions.

Viruses are the dominant form of genetically reproducing entities on Earth. Yet, viruses are mostly neglected in the context of astrobiology due to their non-living nature. In this discussion it is considered whether viruses are likely to be transferred within bacterial endospores to other planetary bodies through lithopanspermia. Interestingly, it seems possible that ecosystems of panspermial origin might yield biospheres in which viruses are absent. The evolutionary pathway of life in these systems might differ significantly from the path observed on Earth. We hypothesize that the difference in the two potential ways for the emergence of life, those being panspermial or local origin, on any certain planet could be clarified by analyzing the diversity of virosphere on the planet. The use of viruses as putative biomarkers is also discussed and studied.

This paper develops a detailed quantitative model which uses the Drake equation and an assumption of an average maximum radio broadcasting distance by an communicative civilization. Using this basis, it estimates the minimum civilization density for contact between two civilizations to be probable in a given volume of space under certain conditions, the amount of time it would take for a first contact, and the question of whether reciprocal contact is possible.

The effect of heat on the reaction system of glycine/aspartic acid and glycine/valine in the aqueous environment as well as in montmorillonite clay suspension with or without divalent cations (Ca2+, Mg2+ and Ni2+) has been investigated at 85°C±5°C for varying periods under prebiotic drying and wetting conditions. The resulting products were analysed and characterized by chromatographic and spectroscopic methods. Peptide formation appears to depend on the duration of heat effect, nature of reactant amino acids and, to some extent, on montmorillonite clay incorporated with divalent cations. In the glycine/aspartic acid system, oligomerization of glycine was limited up to trimer level (Gly)3 along with the formation of glycyl-aspartic acid, while linear and cyclic peptides of aspartic acid were not formed, whereas the glycine/valine system preferentially elongated homo-oligopeptide of glycine up to pentamer level (Gly)5 along with formation of hetero-peptides (Gly-Val and Val-Gly). These studies are relevant in the context of the prebiotic origin of proteins and the role of clay and metal ions in condensation and oligomerization of amino acids. The length of the bio-oligomer chain depends upon the reaction conditions. However, condensation into even a small length seems significant, as the same process would have taken millions of years in the primitive era of the Earth, leading to the first proteins.

Ices in the Martian polar caps are potential habitats for various species of microorganisms. Salts in the ice and biological anti-freeze polymers maintain liquid in cracks in the ices far below 0°C, possibly down to the mean 220–240 K. Sub-surface microbial life is shielded from ultraviolet (UV) radiation, but could potentially be activated on south-facing slopes under the midday, midsummer Sun. Such life would be limited by low levels of vapour, little transport of nutrients, low light levels below a protective dirt-crust, frost accumulation at night and in shadows, and little if any active translocation of organisms. As in the Antarctic and in permafrost, movement to new habitats depends on geo-climatic changes, which for Mars's north polar cap occur on a 50 000 year scale, except for rare meteorite impacts.

The search for extraterrestrial intelligence (SETI) has been heavily influenced by solutions to the Drake Equation, which returns an integer value for the number of communicating civilizations resident in the Milky Way, and by the Fermi Paradox, glibly stated as: ‘If they are there, where are they?’. Both rely on using average values of key parameters, such as the mean signal lifetime of a communicating civilization. A more accurate answer must take into account the distribution of stellar, planetary and biological attributes in the galaxy, as well as the stochastic nature of evolution itself. This paper outlines a method of Monte Carlo realization that does this, and hence allows an estimation of the distribution of key parameters in SETI, as well as allowing a quantification of their errors (and the level of ignorance therein). Furthermore, it provides a means for competing theories of life and intelligence to be compared quantitatively.

Ab initio calculations for scytonemin, an important ultraviolet (UV)-radiation protective biomolecule synthesized by extremophilic cyanobacteria in stressed terrestrial environments, are reported for the first time. Vibrational spectroscopic assignments for the previously studied Raman spectra assist in the identification of the major features in the observed data. Calculations of the electronic absorption spectra confirm the capability of this molecule to absorb in all three regions of the UV, UVA, UVB and UVC, and also illustrate the need for a dimeric species in this respect. The presence of significant steric hindrance between the two halves of the dimeric molecule about the C—C bridging bond in scytonemin forces the molecule significantly out of planarity, contrary to assumptions made in the literature; however, it appears that the monomer is capable of absorbing to only a limited extent in the UVB and UVC regions only, so conferring a special emphasis upon the need for the dimerization to remove the lower-energy UV radiation whilst still affording protection for the chlorophyll with transmission of the visible radiation required for photosynthesis. The observation of vibrational band wavenumber coincidences for the first time between the infrared and Raman spectra confirm the non-planar structural prediction from the calculations. The results of this study provide information about the protective chemical strategies of terrestrial extremophilic cyanobacteria and provide a basis for the search for molecules of this type in the astrobiological exploration of Mars.

A study was undertaken to determine if amber, coal and clay samples contain bacteria, in relation to the possibility that rocks ejected from Earth might contain microorganisms capable of colonizing other planets. A technique for isolating bacteria from rocks was developed which excluded the possibility that any of the rock isolates resulted from contamination. Two species of Bacillus were found in the amber sample, and a species of the same genus was found in coal; bacilli were also commonly found in clay. It is concluded that species of the spore-forming genus Bacillus could therefore be ejected from Earth in these geological substrates and possibly be transferred elsewhere.